- ID:
- ivo://CDS.VizieR/J/other/PSS/53.925
- Title:
- CCD photometry of 23 minor planets
- Short Name:
- J/other/PSS/53.9
- Date:
- 14 Dec 2021 08:11:55
- Publisher:
- CDS
- Description:
- We present CCD photometric observations of 23 main-belt asteroids, of which 8 have never been observed before thus the data of these objects are the first in the literature. The majority showed well detectable light variations, exceeding 0.1m. We have determined synodic periods for 756 Lilliana (9.36),1270 Datura (3.4), 1400 Tirela (13.36), 1503 Kuopio (9.98), 3682 Welther (3.59), 7505 Furushu (4.14) and 11436 1969 QR (2.6), while uncertain period estimates were possible for 469 Argentina (12.3), 546 Herodias (10.4) and 1026 Ingrid (5.3). The shape of the lightcurves of 3682 Welther changed on a short time-scale and showed dimmings that might be attributed to eclipses in a binary system. For the remaining objects, only lower limits of the periods and amplitudes were concluded.
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- ID:
- ivo://CDS.VizieR/J/A+A/652/A141
- Title:
- Chariklo's system from stellar occultations
- Short Name:
- J/A+A/652/A141
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The Centaur (10199) Chariklo has the first rings system discovered around a small object. It was first observed using stellar occultation in 2013. Stellar occultations allow the determination of sizes and shapes with kilometre accuracy and obtain characteristics of the occulting object and its vicinity. Using stellar occultations observed between 2017 and 2020, we aim at constraining Chariklo's and its rings physical parameters. We also determine the rings' structure, and obtain precise astrometrical positions of Chariklo. We predicted and organised several observational campaigns of stellar occultations by Chariklo. Occultation light curves were measured from the data sets, from which ingress and egress times, and rings' width and opacity were obtained. These measurements, combined with results from previous works, allow us to obtain significant constraints on Chariklo's shape and rings' structure. We characterise Chariklo's ring system (C1R and C2R), and obtain radii and pole orientations that are consistent with, but more accurate than, results from previous occultations. We confirmed the detection of W-shaped structures within C1R and an evident variation of radial width. The observed width ranges between 4.8 and 9.1km with a mean value of 6.5km. One dual observation (visible and red) does not reveal any differences in the C1R opacity profiles, indicating ring particle's size larger than a few microns. The C1R ring eccentricity is found to be smaller than 0.022 (3-sigma), and its width variations may indicate an eccentricity higher than 0.005. We fit a tri-axial shape to Chariklo's detections over eleven occultations and determine that Chariklo is consistent with an ellipsoid with semi-axes of 143.8, 135.2 and 99.1km. Ultimately, we provided seven astrometric positions at a milliarcseconds accuracy level, based on Gaia EDR3, and use it to improve Chariklo's ephemeris.
- ID:
- ivo://CDS.VizieR/J/AJ/119/2008
- Title:
- 10199 Chariklo stellar occultation: 1999-2005
- Short Name:
- J/AJ/119/2008
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The Flagstaff Astrometric Scanning Transit Telescope was used to scan the sky in search of occultation candidates through which the Centaur 10199 Chariklo (formerly 1997 CU_26_) will pass in 1999-2005. Positions for 96,397 stars (magnitudes 7.5<V<17.3) were determined using differential reductions to the ACT catalog of star positions and proper motions, and accuracies of +/-30mas were achieved for well-exposed images. The ephemeris for 10199 Chariklo was improved by including the new positions presented in this paper and, second, by correcting older positions taken from the literature for systematic errors. During this time period, 10199 Chariklo passes within 2" of 117 of these stars, which are identified as occultation candidates in this paper. Among these, 28 candidates have magnitudes V<15.0, making them the best choices for observing programs using portable telescopes. Circumstances for each occultation are given. Because the angular radius of 10199 Chariklo is only about 15mas, the astrometry provided in this paper is only accurate enough for identifying possible occultation events and is not sufficient for predicting individual shadow paths across the surface of Earth, although representative cases are given. Last-minute astrometry with a large-aperture telescope will be needed to refine each prediction.
- ID:
- ivo://CDS.VizieR/J/A+A/406/751
- Title:
- Close encounters of asteroids 2003-2020
- Short Name:
- J/A+A/406/751
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Selection have been made of asteroids-asteroids close encounters inducing perturbations large enough to deduce masses of perturbing objects. In tablea1.dat, and tablea3.dat, the epoch of encounters is given as well as the impact parameter, the relative distance and the criterion of maximum deflection (see section 2). The epoch of encounters is defined as the epoch when the relative distance or velocity between the two asteroids become minimum or the criterion of deflection becomes maximum. The ({Delta}{alpha},{Delta}{delta}) given in tables are the maximum differences in right ascension and declination between the perturbed and the unperturbed orbits and the epoch of maximum ({Delta}{alpha},{Delta}{delta}) is defined as the mean epoch for the maximum values of ({Delta}{alpha},{Delta}{delta}). Finally, in tablea2.dat and tablea4.dat, we give the observability of each encounters. We give the periods when the asteroids have a mean solar elongation greater than 50 degrees and when the perturbations of the orbits induced by the Multiple Gravitational Event (MGE) are greater than 50 mas. Mean values of these perturbations in right ascension and declination computed over the corresponding periods are given in Columns 4 and 5.
- ID:
- ivo://CDS.VizieR/J/AJ/157/228
- Title:
- Cold Classical TNOs: LCs & rotational properties
- Short Name:
- J/AJ/157/228
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a survey of the rotational and physical properties of the dynamically low inclination Cold Classical (CC) trans-Neptunian objects (TNOs). The CCs are primordial planetesimals and contain information about our solar system and planet formation over the first 100 million years after the Sun's formation. We obtained partial/complete light curves for 42 CCs. We use statistical tests to derive general properties about the shape and rotational frequency distributions of the CCs and infer that they have slower rotations and are more elongated/deformed than the other TNOs. On the basis of the full light curves, the mean rotational period of the CCs is 9.48+/-1.53 hr compared to 8.45+/-0.58 hr for the rest of the TNOs. About 65% of the TNOs have a light-curve amplitude below 0.2 mag compared to the 36% of CCs with small amplitude. We present the full light curve of one likely contact binary, 2004 VC_131_, with a potential density of 1 g/cm^3^ for a mass ratio of 0.4. We have hints that 2004 MU_8_ and 2004 VU_75_ are perhaps potential contact binaries, on the basis of their sparse light curves, but more data are needed to confirm this finding. Assuming equal-sized binaries, we find that ~10%-25% of the CCs could be contact binaries, suggesting a deficit of contact binaries in this population compared to previous estimates and to the (~40%-50%) possible contact binaries in the Plutino population. These estimates are lower limits and may increase if nonequal-sized contact binaries are considered. Finally, we put in context the results of the New Horizons flyby of 2014 MU_69_.
- ID:
- ivo://CDS.VizieR/J/A+A/546/A115
- Title:
- Colors of minor bodies in outer solar system
- Short Name:
- J/A+A/546/A115
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Photometric colours of Minor Bodies in the Outer Solar System (MBOSS). This compilation is based on over 2000 measurement epoch extracted from over 100 articles, and is fairly complete as of Dec. 2011. The average colours and additional information are available in the first file. The second file lists the code of the references used for each object. The third file lists the actual references in bibTex format. The methods used to select the data and compute the averages are described in the accompanying paper. The updated lists are available online at http://www.eso.org/~ohainaut/MBOSS Average photometric colours of Minor Bodies in the Outer Solar System. The table also lists their physico-dynamical class, the number of measurement epochs included in the average, the absolute R-band magnitude R(1,1,{alpha}), and the slope of the spectroscopic gradient (in %/100nm). are presented in table2.dat. For each MBOSS from table2.dat, table3.dat list of the references from which photometric measurements were used. The table also lists the number of measurement epochs included in the average.
- ID:
- ivo://CDS.VizieR/J/A+A/389/641
- Title:
- Colors of Minor Bodies in the Outer Solar System
- Short Name:
- J/A+A/389/641
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a compilation of all available colors for 104 Minor Bodies in the Outer Solar System (MBOSSes); for each object, the original references are listed. The measurements were combined in a way that does not introduce rotational color artifacts. We then derive the slope, or reddening gradient, of the low resolution reflectance spectra obtained from the broad-band color for each object. A set of color-color diagrams, histograms and cumulative probability functions are presented as a reference for further studies, and are discussed.
- ID:
- ivo://CDS.VizieR/J/ApJS/243/12
- Title:
- Colors of the Outer Solar System Origins Survey
- Short Name:
- J/ApJS/243/12
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The Colours of the Outer Solar System Origins Survey is acquiring near-simultaneous g, r, and J photometry of unprecedented precision with the Gemini North Telescope, targeting nearly 100 trans-Neptunian objects (TNOs) brighter than m_r_=23.6mag discovered in the Outer Solar System Origins Survey. Combining the optical and near-infrared photometry with the well-characterized detection efficiency of the Colours of the Outer Solar System Origins Survey target sample will provide the first flux-limited compositional dynamical map of the outer solar system. In this paper, we describe our observing strategy and detail the data reduction processes we employ, including techniques to mitigate the impact of rotational variability. We present optical and near-infrared colors for 35 TNOs. We find two taxonomic groups for the dynamically excited TNOs, the neutral and red classes, which divide at g-r~0.75. Based on simple albedo and orbital distribution assumptions, we find that the neutral class outnumbers the red class, with a ratio of 4:1 and potentially as high as 11:1. Including in our analysis constraints from the cold classical objects, which are known to exhibit unique albedos and r-z colors, we find that within our measurement uncertainty our observations are consistent with the primordial solar system protoplanetesimal disk being neutral class dominated, with two major compositional divisions in grJ color space.
- ID:
- ivo://CDS.VizieR/J/AJ/157/94
- Title:
- Col-OSSOS: Properties of outer solar system objects
- Short Name:
- J/AJ/157/94
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Both physical and dynamical properties must be considered to constrain the origins of the dynamically excited distant solar system populations. We present high-precision (g-r) colors for 25 small (H_r_>5) dynamically excited trans-Neptunian objects (TNOs) and centaurs acquired as part of the Colours of the Outer Solar System Origins Survey. We combine our data set with previously published measurements and consider a set of 229 colors of outer solar system objects on dynamically excited orbits. The overall color distribution is bimodal and can be decomposed into two distinct classes, termed gray and red, that each has a normal color distribution. The two color classes have different inclination distributions: red objects have lower inclinations than the gray ones. This trend holds for all dynamically excited TNO populations. Even in the worst-case scenario, biases in the discovery surveys cannot account for this trend; it is intrinsic to the TNO population. Considering that TNOs are the precursors of centaurs, and that their inclinations are roughly preserved as they become centaurs, our finding solves the conundrum of centaurs being the only outer solar system population identified so far to exhibit this property. The different orbital distributions of the gray and red dynamically excited TNOs provide strong evidence that their colors are due to different formation locations in a disk of planetesimals with a compositional gradient.
- ID:
- ivo://CDS.VizieR/J/MNRAS/507/4914
- Title:
- Contact-binary (68346) 2001 KZ66 light curves
- Short Name:
- J/MNRAS/507/4914
- Date:
- 19 Jan 2022 09:12:40
- Publisher:
- CDS
- Description:
- The YORP effect is a small thermal-radiation torque experienced by small asteroids, and is considered to be crucial in their physical and dynamical evolution. It is important to understand this effect by providing measurements of YORP for a range of asteroid types to facilitate the development of a theoretical framework. We are conducting a long-term observational study on a selection of near-Earth asteroids to support this. We focus here on (68346) 2001 KZ66, for which we obtained both optical and radar observations spanning a decade. This allowed us to perform a comprehensive analysis of the asteroid's rotational evolution. Furthermore, radar observations from the Arecibo Observatory enabled us to generate a detailed shape model. We determined that (68346) is a retrograde rotator with its pole near the southern ecliptic pole, within a 15-degree radius of longitude 170 degrees and latitude -85-degrees. By combining our radar-derived shape model with the optical light curves we developed a refined solution to fit all available data, which required a YORP strength of (8.43+/-0.69)x10^-8^rad/day/day. (68346) has a distinct bifurcated shape comprising a large ellipsoidal component joined by a sharp neckline to a smaller non-ellipsoidal component. This object likely formed from either the gentle merging of a binary system, or from the deformation of a rubble pile due to YORP spin-up. The shape exists in a stable configuration close to its minimum in topographic variation, where regolith is unlikely to migrate from areas of higher potential.
